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Dead zone accretion flows in protostellar disks

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dc.contributor.author Turner, Neal
dc.contributor.author Sano, T.
dc.date.accessioned 2008-12-03T22:58:35Z
dc.date.available 2008-12-03T22:58:35Z
dc.date.issued 2008-06-01
dc.identifier.citation The Astrophysical Journal Letters, 679: L131–L134, 2008 June 1 DOI: 10.1086/589540 en_US
dc.identifier.clearanceno 08-1354
dc.identifier.uri http://hdl.handle.net/2014/41022
dc.description.abstract Planets form inside protostellar disks in a dead zone where the electrical resistivity of the gas is too high for magnetic forces to drive turbulence. We show that much of the dead zone nevertheless is active and flows toward the star while smooth, large-scale magnetic fields transfer the orbital angular momentum radially outward. Stellar X-ray and radionuclide ionization sustain a weak coupling of the dead zone gas to the magnetic fields, despite the rapid recombination of free charges on dust grains. Net radial magnetic fields are generated in the magnetorotational turbulence in the electrically conducting top and bottom surface layers of the disk, and reach the midplane by ohmic diffusion. A toroidal component to the fields is produced near the midplane by the orbital shear. The process is similar to the magnetization of the solar tachocline. The result is a laminar, magnetically driven accretion flow in the region where the planets form. en_US
dc.description.sponsorship NASA/JPL en_US
dc.language.iso en_US en_US
dc.publisher The American Astronomical Society en_US
dc.subject circumstellar matter en_US
dc.subject instabilities en_US
dc.subject MHD en_US
dc.subject solar system en_US
dc.subject star formation en_US
dc.title Dead zone accretion flows in protostellar disks en_US
dc.type Article en_US


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